Below we compare our results with the lightcurve of SN 2018don [1]} as [2]} did.
The most similar lightcurve shapes to the shape of the lightcurve of SN 2018don are the lightcurves at \(\theta =30^\circ \) , \(\theta =50^\circ \)  and \(\theta =80^\circ \)  in EXP1 with \(\kappa =0.1 {~\rm cm}^2 {~\rm g}^{-1}\)  that we present in the middle panel of Fig. REF .
However, the wide peak duration in these lightcurves is much shorter than that of SN 2018don. We can prolong the wide peak duration by increasing the CSM mass, e.g., four times longer in the lower panel of Fig. REF . However, the shapes of the lightcurves of the cases with larger masses (the three cases that we present in Fig. REF ) are not as similar to the light curve of SN 2018don. To obtain the same shape as in the middle panel of Fig. REF  (case EXP1 with \(\kappa =0.1 {~\rm cm}^2 {~\rm g}^{-1}\) ) and with a longer wide peak we will have to conduct a very extensive search of the parameter space.
For example, we will have to modify also the explosion properties, which are the same in all cases here. Namely, we will have to change in a systematic way the properties of the exploding jets, like their opening angle, energy, and duration. We also will have to consider a CSM that might be lighter in mass and that does not contain a hydrogen-rich gas. These additions are beyond our specific goal here. In future studies that will include also radiative transfer we will scan the parameter space.
